Crab Nebula 19 21 Oct 2009 Reims Neutrino

Crab Nebula 19 -21 Oct 2009, Reims Neutrino Champagne, Low. Nu 2009, Physics Opportunities with Supernova Neutrinos Georg Raffelt, Max-Planck-Institut für Physik, München Low. Nu 2009, 19 -21 Oct 2009, Reims, France

Stellar Collapse and Supernova Explosion Main-sequence Onion structure star Degenerate iron core: r 109 g cm-3 Hydrogen Burning T 1010 K MFe 1. 5 Msun RFe 8000 km Georg Raffelt, Max-Planck-Institut für Physik, München Collapse (implosion) Helium-burning star Helium Burning Hydrogen Burning Low. Nu 2009, 19 -21 Oct 2009, Reims, France

Stellar Collapse and Supernova Explosion Newborn Neutron Star Collapse Explosion (implosion) ~ 50 km Neutrino Cooling Proto-Neutron Star r rnuc = 3 1014 g cm-3 T 30 Me. V Georg Raffelt, Max-Planck-Institut für Physik, München Low. Nu 2009, 19 -21 Oct 2009, Reims, France

Stellar Collapse and Supernova Explosion Newborn Neutron Star ~ 50 km Gravitational binding energy Eb 3 1053 erg 17% MSUN c 2 Neutrino Cooling Proto-Neutron Star r rnuc = 3 1014 g cm-3 T 30 Me. V Georg Raffelt, Max-Planck-Institut für Physik, München This shows up as 99% Neutrinos 1% Kinetic energy of explosion (1% of this into cosmic rays) 0. 01% Photons, outshine host galaxy Neutrino luminosity Ln 3 1053 erg / 3 sec 3 1019 LSUN While it lasts, outshines the entire visible universe Low. Nu 2009, 19 -21 Oct 2009, Reims, France

Diffuse Supernova Neutrino Background (DSNB) Supernova rate approximately 1 SN / 1010 LSun, B / 100 years Lsun, B = 0. 54 Lsun = 2 1033 erg/s En ~ 3 1053 erg per core-collapse Core-collapse neutrino luminosity of typical galaxy comparable to photon luminosity (from nuclear burning) Core-collapse rate somewhat larger in the past. Estimated present-day flux ~ 10 cm-2 s-1 Pushing the boundaries of neutrino astronomy to cosmological distances Beacom & Vagins, hep-ph/0309300 [Phys. Rev. Lett. , 93: 171101, 2004] Georg Raffelt, Max-Planck-Institut für Physik, München Low. Nu 2009, 19 -21 Oct 2009, Reims, France

Neutrino Signal of Supernova 1987 A Kamiokande-II (Japan) Water Cherenkov detector 2140 tons Clock uncertainty 1 min Irvine-Michigan-Brookhaven (US) Water Cherenkov detector 6800 tons Clock uncertainty 50 ms Baksan Scintillator Telescope (Soviet Union), 200 tons Random event cluster ~ 0. 7/day Clock uncertainty +2/-54 s Within clock uncertainties, signals are contemporaneous Georg Raffelt, Max-Planck-Institut für Physik, München Low. Nu 2009, 19 -21 Oct 2009, Reims, France

Large Detectors for Supernova Neutrinos Mini. Boo. NE (200) LVD (400) Borexino (100) Baksan (100) Ice. Cube (106) Georg Raffelt, Max-Planck-Institut für Physik, München Super-Kamiokande (104) Kam. LAND (400) In brackets events for a “fiducial SN” at distance 10 kpc Low. Nu 2009, 19 -21 Oct 2009, Reims, France

Ice. Cube as a Supernova Neutrino Detector Each optical module (OM) picks up Cherenkov light from its neighborhood. SN appears as “correlated noise”. • About 300 Cherenkov photons per OM from a SN at 10 kpc • Noise per OM ~280 Hz • Total of 4800 OMs foreseen in Ice. Cube Georg Raffelt, Max-Planck-Institut für Physik, München Ice. Cube SN signal at 10 kpc, based on a numerical Livermore model [Dighe, Keil & Raffelt, hep-ph/0303210] Method first discussed by • Pryor, Roos & Webster, Ap. J 329: 355 (1988) • Halzen, Jacobsen & Zas astro-ph/9512080 Low. Nu 2009, 19 -21 Oct 2009, Reims, France

Local Group of Galaxies With megatonne class (30 x SK) 60 events from Andromeda Current best neutrino detectors sensitive out to few 100 kpc Georg Raffelt, Max-Planck-Institut für Physik, München Low. Nu 2009, 19 -21 Oct 2009, Reims, France

Core-Collapse SN Rate in the Milky Way SN statistics in external galaxies van den Bergh & Mc. Clure (1994) Cappellaro & Turatto (2000) Gamma rays from 26 Al (Milky Way) Diehl et al. (2006) Historical galactic SNe (all types) Strom (1994) Tammann et al. (1994) No galactic neutrino 90 % CL (25 y obserservation) burst since 1980 Alekseev et al. (1993) 0 1 2 3 4 5 6 7 8 9 10 Core-collapse SNe per century References: van den Bergh & Mc. Clure, Ap. J 425 (1994) 205. Cappellaro & Turatto, astroph/0012455. Diehl et al. , Nature 439 (2006) 45. Strom, Astron. Astrophys. 288 (1994) L 1. Tammann et al. , Ap. J 92 (1994) 487. Alekseev et al. , JETP 77 (1993) 339 and my update. Georg Raffelt, Max-Planck-Institut für Physik, München Low. Nu 2009, 19 -21 Oct 2009, Reims, France

Observed SNe in the Local Universe (Past Decade) Statistical Prediction Kistler, Yüksel, Ando, Beacom & Suzuki, ar. Xiv: 0810. 1959 Georg Raffelt, Max-Planck-Institut für Physik, München Low. Nu 2009, 19 -21 Oct 2009, Reims, France

Looking forward Probing Supernova Physics Georg Raffelt, Max-Planck-Institut für Physik, München Low. Nu 2009, 19 -21 Oct 2009, Reims, France

Delayed Explosion Wilson, Proc. Univ. Illinois Meeting on Num. Astrophys. (1982) Bethe & Wilson, Ap. J 295 (1985) 14 Georg Raffelt, Max-Planck-Institut für Physik, München Low. Nu 2009, 19 -21 Oct 2009, Reims, France

Exploding Models (8 -10 Solar Masses) with O-Ne-Mg-Cores Kitaura, Janka & Hillebrandt: “Explosions of O-Ne-Mg cores, the Crab supernova, and subluminous type II-P supernovae”, astro-ph/0512065 Georg Raffelt, Max-Planck-Institut für Physik, München Low. Nu 2009, 19 -21 Oct 2009, Reims, France

Neutrino Signal from an O-Ne-Mg Core SN (Garching) Georg Raffelt, Max-Planck-Institut für Physik, München Low. Nu 2009, 19 -21 Oct 2009, Reims, France

New Long-Term Cooling Calculations (Basel Group) Fischer et al. (Basel Group), ar. Xiv: 0908. 1871 Georg Raffelt, Max-Planck-Institut für Physik, München Low. Nu 2009, 19 -21 Oct 2009, Reims, France

Flavor Dependence of Neutrino Emission (Basel Group) Fischer et al. (Basel Group), ar. Xiv: 0908. 1871 Georg Raffelt, Max-Planck-Institut für Physik, München Low. Nu 2009, 19 -21 Oct 2009, Reims, France

Standing Accretion Shock Instability (SASI) Mezzacappa et al. , http: //www. phy. ornl. gov/tsi/pages/simulations. html Georg Raffelt, Max-Planck-Institut für Physik, München Low. Nu 2009, 19 -21 Oct 2009, Reims, France

Luminosity Variation Detectable in Neutrinos? Polar direction Hemispheric average Neutrino events in 10 ms bins for SN (10 kpc) during accretion phase: • Super-K 70 • 30 x Super-K 2 103 • Ice. Cube 1 104 1 s ~ 10% 1 s ~ 2% 1 s ~ 1% Detecting the spectrum of luminosity variations can • Detect SASI instability in neutrinos • Provide equation-of-state information Marek, Janka & Müller, ar. Xiv: 0808. 4136 Georg Raffelt, Max-Planck-Institut für Physik, München Low. Nu 2009, 19 -21 Oct 2009, Reims, France

Fourier Transform of Luminosity Variation Polar direction Hemispheric average Approximate level of Poisson noise in Ice. Cube for a SN at 10 kpc Detectability to be studied in more detail (Lund, Marek, Lunardini, Janka, Raffelt, Work in progress) Marek, Janka & Müller, ar. Xiv: 0808. 4136 Georg Raffelt, Max-Planck-Institut für Physik, München Low. Nu 2009, 19 -21 Oct 2009, Reims, France

Neutrino Mass and Resolution of Time Variations Signal dispersion for Next Nearby SN • Ice. Cube binning of data: 1. 64 ms in each OM • Laboratory neutrino mass limit: 2. 2 e. V • Cosmological limit Smn < 0. 6 e. V, so individual mass limit 0. 2 e. V • KATRIN sensitivity roughly 0. 2 e. V For SN signal interpretation of fast time variations, it is important to have the cosmological limit and future KATRIN measurement/limit Supernova neutrino aficionados are new customers for KATRIN results! Georg Raffelt, Max-Planck-Institut für Physik, München Low. Nu 2009, 19 -21 Oct 2009, Reims, France

Gravitational Waves from Core-Collapse Supernovae Müller, Rampp, Buras, Janka, & Shoemaker, “Towards gravitational wave signals from realistic core collapse supernova models, ” astro-ph/0309833 Asymmetric neutrino emission Bounce Convection The gravitational-wave signal from convection is a generic and dominating feature Georg Raffelt, Max-Planck-Institut für Physik, München Low. Nu 2009, 19 -21 Oct 2009, Reims, France

Millisecond Bounce Time Reconstruction Super-Kamiokande • Emission model adapted to measured SN 1987 A data • “Pessimistic distance” of 20 kpc Ice. Cube Onset of neutrino emission • Determine bounce time to within a few tens of milliseconds Pagliaroli, Vissani, Coccia & Fulgione ar. Xiv: 0903. 1191 Georg Raffelt, Max-Planck-Institut für Physik, München 10 kpc Halzen & Raffelt ar. Xiv: 0908. 2317 Low. Nu 2009, 19 -21 Oct 2009, Reims, France

Looking forward Neutrino Flavor Oscillations Georg Raffelt, Max-Planck-Institut für Physik, München Low. Nu 2009, 19 -21 Oct 2009, Reims, France

Level-Crossing Diagram in a SN Envelope Normal mass hierarchy Inverted mass hierarchy Dighe & Smirnov, Identifying the neutrino mass spectrum from a supernova neutrino burst, astro-ph/9907423 Georg Raffelt, Max-Planck-Institut für Physik, München Low. Nu 2009, 19 -21 Oct 2009, Reims, France

Collective Effects in Neutrino Flavor Oscillations Collapsed supernova core or accretion torus of merging neutron stars: • Neutrino flux very dense: Up to 1035 cm-3 • Neutrino-neutrino interaction energy much larger than vacuum oscillation frequency • Large “matter effect” of neutrinos on each other • Non-linear oscillation effects • Assume 80% anti-neutrinos • Vacuum oscillation frequency w = 0. 3 km-1 • Neutrino-neutrino interaction energy at nu sphere (r = 10 km) m = 0. 3 105 km-1 • Falls off approximately as r-4 (geometric flux dilution and nus become more co-linear) Georg Raffelt, Max-Planck-Institut für Physik, München Low. Nu 2009, 19 -21 Oct 2009, Reims, France

Collective SN Neutrino Oscillations since 2006 Two seminal papers in 2006 triggered a torrent of activities Duan, Fuller, Qian, astro-ph/0511275, Duan et al. astro-ph/0606616 Duan, Fuller, Carlson & Qian, astro-ph/0608050, 0703776, ar. Xiv: 0707. 0290, 0710. 1271. Duan, Fuller & Qian, ar. Xiv: 0706. 4293, 0801. 1363, 0808. 2046. Duan, Fuller & Carlson, ar. Xiv: 0803. 3650. Duan & Kneller, ar. Xiv: 0904. 0974. Hannestad, Raffelt, Sigl & Wong, astro-ph/0608695. Balantekin & Pehlivan, astro-ph/0607527. Balantekin, Gava & Volpe, ar. Xiv: 0710. 3112. Gava & Volpe, ar. Xiv: 0807. 3418. Gava, Kneller, Volpe & Mc. Laughlin, ar. Xiv: 0902. 0317. Raffelt & Sigl, hep-ph/0701182. Raffelt & Smirnov, ar. Xiv: 0705. 1830, 0709. 4641. Esteban-Pretel, Pastor, Tomàs, Raffelt & Sigl, ar. Xiv: 0706. 2498, 0712. 1137. Esteban-Pretel, Mirizzi, Pastor, Tomàs, Raffelt, Serpico & Sigl, ar. Xiv: 0807. 0659. Raffelt, ar. Xiv: 0810. 1407. Fogli, Lisi, Marrone & Mirizzi, ar. Xiv: 0707. 1998. Fogli, Lisi, Marrone & Tamborra, ar. Xiv: 0812. 3031, 0907. 5115. Lunardini, Müller & Janka, ar. Xiv: 0712. 3000. Dasgupta & Dighe, ar. Xiv: 0712. 3798. Dasgupta, Dighe & Mirizzi, ar. Xiv: 0802. 1481. Dasgupta, Dighe, Mirizzi & Raffelt, ar. Xiv: 0801. 1660, 0805. 3300. Dasgupta, Dighe, Raffelt & Smirnov, ar. Xiv: 0904. 3542. Sawyer, ar. Xiv: 0803. 4319. Chakraborty, Choubey, Dasgupta & Kar, ar. Xiv: 0805. 3131. Blennow, Mirizzi & Serpico, ar. Xiv: 0810. 2297. Wei Liao, ar. Xiv: 0904. 0075, 0904. 2855. Georg Raffelt, Max-Planck-Institut für Physik, München Low. Nu 2009, 19 -21 Oct 2009, Reims, France

Spectral Split (Accretion-Phase Example) Initial fluxes at neutrino sphere For explanation see After collective transformation Raffelt & Smirnov ar. Xiv: 0705. 1830 0709. 4641 Duan, Fuller, Carlson & Qian ar. Xiv: 0706. 4293 0707. 0290 Fogli, Lisi, Marrone & Mirizzi, ar. Xiv: 0707. 1998 Georg Raffelt, Max-Planck-Institut für Physik, München Low. Nu 2009, 19 -21 Oct 2009, Reims, France

Distinguishing Mixing Scenarios Survival Probability Hierarchy Earth effects sin 2 Q 13 E < Esplit Normal Inverted ≳ 10 -3 ≲ 10 -5 0 sin 2 Q 12 E > Esplit 0 cos 2 Q 12 sin 2 Q 12 0 0 - • Assuming “standard” flux spectra leading to a single split • Probably generic for accretion phase Adapted from Dighe, ar. Xiv: 0809. 2977 Georg Raffelt, Max-Planck-Institut für Physik, München Low. Nu 2009, 19 -21 Oct 2009, Reims, France

Mass Hierarchy at Extremely Small Theta-13 Using Earth matter effects to diagnose transformations Ratio of spectra in two water Cherenkov detectors (0. 4 Mton), one shadowed by the Earth, the other not Dasgupta, Dighe & Mirizzi, ar. Xiv: 0802. 1481 Georg Raffelt, Max-Planck-Institut für Physik, München Low. Nu 2009, 19 -21 Oct 2009, Reims, France

Looking forward What exactly will be learnt from the neutrinos of the next nearby SN depends a lot on what exactly is observed Georg Raffelt, Max-Planck-Institut für Physik, München Low. Nu 2009, 19 -21 Oct 2009, Reims, France

Looking forward SN neutrinos are powerful astrophysical and particle-physics messengers Georg Raffelt, Max-Planck-Institut für Physik, München Low. Nu 2009, 19 -21 Oct 2009, Reims, France